  Using only physical mechanisms, i.e., 3D MHD with no phenomenological
viscosity, we have simulated the dynamics of a moderately thin accretion disk
subject to torques whose radial scaling mimics those produced by lowest-order
post-Newtonian gravitomagnetism. In this simulation, we have shown how, in the
presence of MHD turbulence, a time-steady transition can be achieved between an
inner disk region aligned with the equatorial plane of the central mass's spin
and an outer region orbiting in a different plane. The position of the
equilibrium orientation transition is determined by a balance between
gravitomagnetic torque and warp-induced inward mixing of misaligned angular
momentum from the outer disk. If the mixing is interpreted in terms of
diffusive transport, the implied diffusion coefficient is
~(0.6--0.8)c_s^2/Omega for sound speed c_s and orbital frequency Omega. This
calibration permits estimation of the orientation transition's equilibrium
location given the central mass, its spin parameter, and the disk's surface
density and scaleheight profiles. However, the alignment front overshoots
before settling into an equilibrium, signaling that a diffusive model does not
fully represent the time-dependent properties of alignment fronts under these
conditions. Because the precessional torque on the disk at the alignment front
is always comparable to the rate at which misaligned angular momentum is
brought inward to the front by warp-driven radial motions, no break forms
between the inner and outer portions of the disk in our simulation. Our results
also raise questions about the applicability to MHD warped disks of the
traditional distinction between "bending wave" and "diffusive" regimes.
