Multidimensional hydrodynamic simulations of shell convection in massive stars suggest the development of aspherical perturbations that may be amplified during iron core-collapse. These perturbations have a crucial and qualitative impact on the delayed neutrino-driven core-collapse supernova explosion mechanism by increasing the total stress behind the stalled shock. In this paper, we investigate the properties of a 15 msun model evolved in 1-,2-, and 3-dimensions (3D) for the final $sim$424 seconds before gravitational instability and iron core-collapse using MESA and the FLASH simulation framework. We find that just before collapse, our initially perturbed fully 3D model reaches angle-averaged convective velocity magnitudes of $approx$ 240-260 km s$^{-1}$ in the Si- and O-shell regions with a Mach number $approx$ 0.06. We find the bulk of the power in the O-shell resides at large scales, characterized by spherical harmonic orders ($ell$) of 2-4, while the Si-shell shows broad spectra on smaller scales of $ellapprox30-40$. Both convective regions show an increase in power at $ell=5$ near collapse. We show that the 1D texttt{MESA} model agrees with the convective velocity profile and speeds of the Si-shell when compared to our highest resolution 3D model. However, in the O-shell region, we find that texttt{MESA} predicts speeds approximately emph{four} times slower than all of our 3D models suggest. All eight of the multi-dimensional stellar models considered in this work are publicly available.
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