Context. Magnetic reconnection in the solar atmosphere drives energetic phenomena, such as Ellerman bombs, UV bursts, and surges. Aims. Our aim is to employ high-resolution observations to advance the general understanding of such phenomena and their mutual connections. Methods. We used coordinated observations from Swedish 1-m Solar Telescope (SST), Interface Region Imaging Spectrograph (IRIS), Solar Dynamics Observatory (SDO), and Hinode/X-ray Telescope (XRT) to analyze an active region with strong and repeated magnetic flux emergence. This region displayed long-duration UV burst activity, the occurrence of multiple Ellerman bombs, and the recurrent ejection of surges. Results. Chromospheric imaging in the Hα and Hβ lines indicates the presence of a dome-like structure that overarches the region where magnetic flux is emerging into the photosphere. The curved chromospheric fibrils are closely associated with bright and similarly curved extensions from a UV burst in the IRIS 1400 Å channel. We observed an episode of formation of a bright sheet along the curved fibrils in Hβ that subsequently fragmented into plasmoid-like blobs, with peak emission at a Doppler offset of +43 km s-1. IRIS Si IV lines in the same region show complex and non-Gaussian line profiles that display asymmetric extensions to high Doppler offsets. Some profiles have clear components with Doppler offsets in excess of 150 km s-1 on both sides of the nominal line center. The optically thin SDO/AIA channels, including 94 Å, show intermittent and repeated occurrences of the burst. Emission measure and filter ratio analysis indicate that the burst is multi-thermal and can attain temperatures beyond 1 MK. AIA and Hinode/XRT observations reveal a localized EUV and soft-X-ray counterpart of the burst-and-dome system, supporting the presence of intrinsically multithermal plasma that reaches coronal, and likely multi-million Kelvin, temperatures. Conclusions. Our observations resolved aspects of the interaction between emerging magnetic field and the overlying pre-existing fields. To fully trace the rise of magnetic fields through the atmosphere and characterize its various forms of associated energy release processes, a continued and coordinated effort of acquisition of diagnostics across a wide range of wavelengths is required.