Recent studies have established magnetized disk winds as the primary mechanism driving accretion and evolution in protoplanetary disks (PPDs), which can co-exist with turbulence from the magneto-rotational instability (MRI) in the outer disk. We conduct 3D global non-ideal magnetohydrodynamic (MHD) simulations of type-II planet-disk interaction that both properly resolve the MRI turbulence and accommodate the MHD disk wind. We found that the planet triggers the poloidal magnetic flux concentration around its orbit, likely associated with spiral density shocks. The concentrated magnetic flux strongly enhances angular momentum removal in the gap region and alters the torque balance, making the planet-induced gap shape more similar to an inviscid disk, while being much deeper. The gap region is characterized by a fast trans-sonic accretion flow that is asymmetric in azimuth about the planet and lacking the horseshoe turns. Further zooming in around the planet reveals the formation of a circumplanetary disk, which is fed by infall from the polar region whereas angular momentum transport is governed by magnetic stresses.