  This paper presents a continuation of our efforts to numerically study
accretion disks that are misaligned (tilted) with respect to the rotation axis
of a Kerr black hole. Here we present results of a global numerical simulation
which fully incorporates the effects of the black hole spacetime as well as
magnetorotational turbulence that is the primary source of angular momentum
transport in the flow. This simulation shows dramatic differences from
comparable simulations of untilted disks. Accretion onto the hole occurs
predominantly through two opposing plunging streams that start from high
latitudes with respect to both the black-hole and disk midplanes. This is due
to the aspherical nature of the gravitational spacetime around the rotating
black hole. These plunging streams start from a larger radius than would be
expected for an untilted disk. In this regard the tilted black hole effectively
acts like an untilted black hole of lesser spin. Throughout the duration of the
simulation, the main body of the disk remains tilted with respect to the
symmetry plane of the black hole; thus there is no indication of a
Bardeen-Petterson effect in the disk at large. The torque of the black hole
instead principally causes a global precession of the main disk body. In this
simulation the precession has a frequency of $3 (M_\odot/M)$ Hz, a value
consistent with many observed low-frequency quasi-periodic oscillations.
However, this value is strongly dependent on the size of the disk, so this
frequency may be expected to vary over a large range.
