  The orbital architectures of short-period exoplanet systems are shaped by
tidal dissipation in their host stars. For low-mass M-dwarfs whose dynamical
tidal response comprises a dense spectrum of inertial modes at low frequencies,
resolving the frequency dependence of tidal dissipation is crucial to capturing
the effect of tides on planetary orbits throughout the evolutionary stages of
the host star. We use non-perturbative spectral methods to calculate the normal
mode oscillations of a fully-convective M-dwarf modeled using realistic stellar
profiles from MESA. We compute the dissipative tidal response composed of
contributions from each mode as well as non-adiabatic coupling between the
modes, which we find to be an essential component of the dissipative
calculations. Using our results for dissipation, we then compute of the
evolution of circular, coplanar planetary orbits under the influence of tides
in the host star. We find that orbital migration driven by resonance locking
affects the orbits of Earth-mass planets at orbital periods $P_{\rm orb}
\lesssim 1.5$ day and of Jupiter-mass planets at $P_{\rm orb} \lesssim 2.5$
day. Due to resonantly-driven orbital decay and outward migration, we predict a
dearth of small planets closer than $P_{\rm orb} \sim 1$ day and similarly
sparse numbers of more massive planets out to $P_{\rm orb} \sim 3$ day.
