  We study tidal dissipation in models of rotating giant planets with masses in
the range $0.1 - 10 M_\mathrm{J}$ throughout their evolution. Our models
incorporate a frequency-dependent turbulent effective viscosity acting on
equilibrium tides (including its modification by rapid rotation consistent with
hydrodynamical simulations) and inertial waves in convection zones, and
internal gravity waves in the thin radiative atmospheres. We consider a range
of planetary evolutionary models for various masses and strengths of stellar
instellation. Dissipation of inertial waves is computed using a
frequency-averaged formalism fully accounting for planetary structures.
Dissipation of gravity waves in the radiation zone is computed assuming these
waves are launched adiabatically and are subsequently fully damped (by wave
breaking/radiative damping). We compute modified tidal quality factors $Q'$ and
evolutionary timescales for these planets as a function of their ages. We find
inertial waves to be the dominant mechanism of tidal dissipation in giant
planets whenever they are excited. Their excitation requires the tidal period
($P_\mathrm{tide}$) to be longer than half the planetary rotation
($P_\mathrm{rot}/2$), and we predict inertial waves to provide a typical
$Q'\sim 10^3 (P_\mathrm{rot}/1 \mathrm{d})^2$, with values between $10^5$ and
$10^6$ for a 10-day period. We show correlations of observed exoplanet
eccentricities with tidal circularisation timescale predictions, highlighting
the key role of planetary tides. A major uncertainty in planetary models is the
role of stably-stratified layers resulting from compositional gradients, which
we do not account for here, but which could modify predictions for tidal
dissipation rates.
