  Global three dimensional magnetohydrodynamic (MHD) simulations of turbulent
accretion disks are presented which start from fully equilibrium initial
conditions in which the magnetic forces are accounted for and the induction
equation is satisfied. The local linear theory of the magnetorotational
instability (MRI) is used as a predictor of the growth of magnetic field
perturbations in the global simulations. The linear growth estimates and global
simulations diverge when non-linear motions - perhaps triggered by the onset of
turbulence - upset the velocity perturbations used to excite the MRI. The
saturated state is found to be independent of the initially excited MRI mode,
showing that once the disk has expelled the initially net flux field and
settled into quasi-periodic oscillations in the toroidal magnetic flux, the
dynamo cycle regulates the global saturation stress level. Furthermore,
time-averaged measures of converged turbulence, such as the ratio of magnetic
energies, are found to be in agreement with previous works. In particular, the
globally averaged stress normalized to the gas pressure, <\alpha_{\rm P}> =
0.034, with notably higher values achieved for simulations with higher
azimuthal resolution. Supplementary tests are performed using different
numerical algorithms and resolutions. Convergence with resolution during the
initial linear MRI growth phase is found for 23-35 cells per scaleheight (in
the vertical direction).
