  Gravito-inertial waves are excited at the interface of convective and
radiative regions and by the Reynolds stresses in the bulk of the convection
zones of rotating stars and planets. Such waves have notable asteroseismic
signatures in the frequency spectra of rotating stars, particularly among
rapidly rotating early-type stars, which provides a means of probing their
internal structure and dynamics. They can also transport angular momentum,
chemical species, and energy from the excitation region to where they dissipate
in radiative regions. To estimate the excitation and convective parameter
dependence of the amplitude of those waves, a monomodal model for stellar and
planetary convection as described in Paper I is employed, which provides the
magnitude of the rms convective velocity as a function of rotation rate. With
this convection model, two channels for wave driving are considered: excitation
at a boundary between convectively stable and unstable regions and excitation
due to Reynolds-stresses. Parameter regimes are found where the sub-inertial
waves may carry a significant energy flux, depending upon the convective Rossby
number, the interface stiffness, and the wave frequency. The super-inertial
waves can also be enhanced, but only for convective Rossby numbers near unity.
Interfacially excited waves have a peak energy flux near the lower cutoff
frequency when the convective Rossby number of the flows that excite them are
below a critical Rossby number that depends upon the stiffness of the
interface, whereas that flux decreases when the convective Rossby number is
larger than this critical Rossby number.
