  The mechanisms of angular momentum transport and level of turbulence in
protoplanetary disks (PPDs) are crucial for understanding many aspects of
planet formation. In the recent years, it has been realized that the
magneto-rotational instability (MRI) tends to be suppressed in PPDs due to
non-ideal MHD effects, and the disk is largely laminar with accretion driven by
magnetized disk winds. In parallel, several hydrodynamical mechanisms have been
identified that likely also generate vigorous turbulence and drive disk
accretion. We study the interplay between MHD winds in PPDs with the vertical
shear instability (VSI), one of the most promising hydrodynamical mechanisms,
through 2D global non-ideal MHD simulations with ambipolar diffusion and Ohmic
resistivity. We find that for typical disk parameters, MHD winds can coexist
with the VSI with accretion primarily wind-driven accompanied by vigorous VSI
turbulence. The properties of the VSI remain similar to unmagnetized case, and
the wind and overall field configuration are not strongly affected by VSI
turbulence, showing modest level of variability and corrugation of midplane
current sheet. Enhanced coupling between gas and magnetic field weakens the
VSI. The VSI is also weakened with increasing magnetization, and we find that
corrugation motions characteristic of the VSI transitions to low-amplitude
breathing mode oscillations.
