The Parker model for coronal heating is investigated through a high resolution simulation. An inertial range is resolved where fluctuating magnetic energy EM(k⊥)∝k⊥-2.7 exceeds kinetic energy EK(k⊥)∝k⊥-0.6. Increments scale as δbℓ≃ℓ-0.85andδuℓ≃ℓ+0.2 with velocity increasing at small scales, indicating that magnetic reconnection plays a prime role in this turbulent system. We show that spectral energy transport is akin to standard magnetohydrodynamic (MHD) turbulence even for a system of reconnecting current sheets sustained by the boundary. In this new MHD turbulent cascade, kinetic energy flows are negligible while cross-field flows are enhanced, and through a series of “reflections” between the two fields, cascade more than half of the total spectral energy flow.