  Protoplanetary disks are dispersed by viscous evolution and photoevaporation
in a few million years; in the interim small, sub-micron sized dust grains must
grow and form planets. The time-varying abundance of small grains in an
evolving disk directly affects gas heating by far-ultraviolet photons, while
dust evolution affects photoevaporation by changing the disk opacity and
resulting penetration of FUV photons in the disk. Photoevaporative flows, in
turn, selectively carry small dust grains leaving the larger particles---which
decouple from the gas---behind in the disk. We study these effects by
investigating the evolution of a disk subject to viscosity, photoevaporation by
EUV, FUV and X-rays, dust evolution, and radial drift using a 1-D multi-fluid
approach (gas + different dust grain sizes) to solve for the evolving surface
density distributions. The 1-D evolution is augmented by 1+1D models
constructed at each epoch to obtain the instantaneous disk structure and
determine photoevaporation rates. The implementation of a dust
coagulation/fragmentation model results in a marginal decrease in disk
lifetimes when compared to models with no dust evolution; the disk lifetime is
thus found to be relatively insensitive to the evolving dust opacity. We find
that photoevaporation can cause significant reductions in the gas/dust mass
ratio in the planet-forming regions of the disk as it evolves, and may result
in a corresponding increase in heavy element abundances relative to hydrogen.
We discuss implications for theories of planetesimal formation and giant planet
formation, including the formation of gas-poor giants. After gas disk
dispersal, $\sim 3\times 10^{-4}$ \ms\ of mass in solids typically remain,
comparable to the solids inventory of our solar system.
