  Formation of the first planetesimals remains an unsolved problem. Growth by
sticking must initiate the process, but multiple studies have revealed a series
of barriers that can slow or stall growth, most of them due to nebula
turbulence. In a companion paper, we study the influence of these barriers on
models of fractal aggregate and solid, compact particle growth in a viscously
evolving solar-like nebula for a range of turbulent intensities
$\alpha_{\rm{t}} = 10^{-5}-10^{-2}$. Here, we examine how disk composition in
these same models changes with time. We find that advection and diffusion of
small grains and vapor, and radial inward drift for larger compact particles
and fractal aggregates, naturally lead to diverse outcomes for planetesimal
composition. Larger particles can undergo substantial inward radial migration
due to gas drag before being collisionally fragmented or partially evaporating
at various temperatures. This leads to enhancement of the associated volatile
in both vapor inside, and solids outside, their respective evaporation fronts,
or ``snowlines''. In cases of lower $\alpha_{\rm{t}}$, we see narrow belts of
volatile or supervolatile material develop in the outer nebula, which could be
connected to the bands of ``pebbles" seen by ALMA. Volatile bands, which
migrate inwards as the disk cools, can persist over long timescales as their
gas phase continues to advect or diffuse outward across its evaporation front.
These belts could be sites where supervolatile-rich planetesimals form, such as
the rare CO-rich and water-poor comets; giant planets formed just outside the
H$_2$O snowline may be enhanced in water.
