  We consider the inner $\sim$ AU of a protoplanetary disk (PPD), at a stage
where angular momentum transport is driven by the mixing of a radial magnetic
field into the disk from a T-Tauri wind. Because the radial profile of the
imposed magnetic field is well constrained, a deterministic calculation of the
disk mass flow becomes possible. The vertical disk profiles obtained in Paper I
imply a stronger magnetization in the inner disk, faster accretion, and a
secular depletion of the disk material. Inward transport of solids allows the
disk to maintain a broad optical absorption layer even when the grain abundance
becomes too small to suppress its ionization. Thus a PPD may show a strong
middle-to-near infrared spectral excess even while its mass profile departs
radically from the minimum-mass solar nebula. The disk surface density is
buffered at $\sim 30$ g cm$^{-2}$: below this, X-rays trigger strong enough
magnetorotational turbulence at the midplane to loft mm-cm sized particles high
in the disk, followed by catastrophic fragmentation. A sharp density gradient
bounds the inner depleted disk, and propagates outward to $\sim 1$-2 AU over a
few Myr. Earth-mass planets migrate through the inner disk over a similar
timescale, whereas the migration of Jupiters is limited by the supply of gas.
Gas-mediated migration must stall outside 0.04 AU, where silicates are
sublimated and the disk shifts to a much lower column. A transition disk
emerges when the dust/gas ratio in the MRI-active layer falls below $X_d \sim
10^{-6}(a_d/\mu{\rm m})$, where $a_d$ is the grain size.
