  Ices are an important constituent of protoplanetary disks. New observational
facilities, notably the James Webb Space Telescope (JWST), will greatly enhance
our view of disk ices by measuring their infrared spectral features. We present
a suite of models to complement these upcoming observations. Our models use a
kinetics-based gas-grain chemical evolution code to simulate the distribution
of ices in a disk, followed by a radiative transfer code using a subset of key
ice species to simulate the observations. We present models reflecting both
molecular inheritance and chemical reset initial conditions. We find that
near-to-mid-IR absorption features of H$_2$O, CO$_2$, and CH$_3$OH are readily
observable in disk-integrated spectra of highly inclined disks while CO,
NH$_3$, and CH$_4$ ice do not show prominent features. CH$_3$OH ice has low
abundance and is not observable in the reset model, making this species an
excellent diagnostic of initial chemical conditions. CO$_2$ ice features
exhibit the greatest change over disk lifetime, decreasing and increasing for
the inheritance and reset models, respectively. Spatially resolved spectra of
edge-on disks, possible with JWST's integral field unit observing modes, are
ideal for constraining the vertical distribution of ices and may be able to
isolate features from ices closer to the midplane (e.g., CO) given sufficient
sensitivity. Spatially-resolved spectra of face-on disks can trace
scattered-light features from H$_2$O, CO$_2$, and CH$_3$OH, plus CO and CH$_4$
from the outermost regions. We additionally simulate far-IR H$_2$O ice emission
features and find they are strongest for disks viewed face-on.
