  We present results from a pair of high resolution, long timescale ($\sim10^5
GM/c^3$), global, three dimensional magnetohydrodynamical accretion disk
simulations with differing initial magnetic plasma $\beta$ in order to study
the effects of initial toroidal field strength on production of large-scale
poloidal field. We initialize our disks in approximate equilibrium with purely
toroidal magnetic fields of strength $\beta_0=5$ and $\beta_0=200$. We also
perform a limited resolution study. We find that simulations of differing field
strength diverge early in their evolution and remain distinct over the time
studied, indicating that initial magnetic conditions leave a persistent imprint
in our simulations. Neither simulation enters the Magnetically Arrested Disk
(MAD) regime. Both simulations are able to produce poloidal fields from
initially-toroidal fields, with the $\beta_0=5$ simulation evolving clear signs
of a large-scale poloidal field. We make a cautionary note that computational
artifacts in the form of large-scale vortices may be introduced in the
combination of initially-weak field and disk-internal mesh refinement
boundaries, as evidenced by the production of an $m=1$ mode overdensity in the
weak field simulation. Our results demonstrate that the initial toroidal field
strength plays a vital role in simulated disk evolution for the models studied.
