We present results from deep MUSE data in extended mode obtained for three planetary nebulae (PNe) with previously reported high abundance discrepancy factors (ADF). The spatially resolved emission maps of recombination lines (ORLs) and collisionally excited lines (CELs) of oxygen ions point to two different plasma components: one hot component with standard metallicity, and a much cooler plasma with a highly enhanced content of heavy elements relative to hydrogen. We have automatically measured the spatial flux distribution for dozens of emission lines on each object. With the resulting cubes, we construct spatially-resolved maps of the electron density and temperature (from several diagnostics) for each PN, the ionic abundances, and the O++ abundance discrepancy. In all objects, the abundance discrepancy clearly peaks in the central part of the nebula, in agreement with previous findings from long-slit spectra. Two of the analyzed PNe (NGC 6778 and Hf 2-2) have confirmed post-common-envelope binary central stars, the evolution of which has increasingly been linked to the high-ADF phenomenon in PNe. We also find evidence of strong contribution of recombination emission to the auroral [N II] and [O II] lines, emphasizing the importance of taking this effect into account when analyzing data from this type of PN.