The overall structure of the evolving protoplanetary disk is set by the interaction of accretion and dispersal processes such as turbulence, winds and photoevaporation (Ercolano & Pascucci 2017), with finer structural details (as gaps, cavities, spirals and warps) in the disk provided by planet formation (eg. Van der Marel et al. 2015). Recent meteoritic evidence from Kruijer et al. (2017) strongly suggest the presence of two distinct isotopic reservoirs in the <1 Myr solar nebula likely created when Jupiter's formation opened a gap in the disk and separated the nebula into two regions. In this talk, we explore the interdependence of disk structure, accretion and chemistry. We model the radial motions of water vapor and small icy solids in the nebular gas under different assumptions of turbulence and track the bulk water content across heliocentric distance. We then include the formation of a proto-Jupiter within our models and back-track the structure of the solar nebula at various times from spatial and temporal cosmochemical data and constrain the variation of the turbulence paramater $\alpha$. We find that our solar nebula likely had a more turbulent inner disk and a weakly turbulent outer disk, and thus may have been wind-driven. We also find that the solar nebula was likely a transitional disk by 4 Myr. Moreover, we speculate that $\Sigma(r)$ can be a diagnostic of $\alpha(r)$ and therefore, the mechanism of angular momentum transport in the disk.