  The gas dynamics of weakly ionized protoplanetary disks (PPDs) is largely
governed by the coupling between gas and magnetic fields, described by three
non-ideal magnetohydrodynamical (MHD) effects (Ohmic, Hall, ambipolar).
Previous local simulations incorporating these processes have revealed that the
inner regions of PPDs are largely laminar accompanied by wind-driven accretion.
We conduct 2D axisymmetric, fully global MHD simulations of these regions
($\sim1-20$ AU), taking into account all non-ideal MHD effects, with tabulated
diffusion coefficients and approximate treatment of external ionization and
heating. With net vertical field aligned with disk rotation, the Hall-shear
instability strongly amplifies horizontal magnetic field, making the overall
dynamics dependent on initial field configuration. Following disk formation,
the disk likely relaxes into an inner zone characterized by asymmetric field
configuration across the midplane that smoothly transitions to a more symmetric
outer zone. Angular momentum transport is driven by both MHD winds and laminar
Maxwell stress, with both accretion and decretion flows present at different
heights, and modestly asymmetric winds from the two disk sides. With
anti-aligned field polarity, weakly magnetized disks settle into an asymmetric
field configuration with supersonic accretion flow concentrated at one side of
disk surface, and highly asymmetric winds between the two disk sides. In all
cases, the wind is magneto-thermal in nature characterized by mass loss rate
exceeding the accretion rate. More strongly magnetized disks give more
symmetric field configuration and flow structures. Deeper far-UV penetration
leads to stronger and less stable outflows. Implications for observations and
planet formation are also discussed.
