  Gravito-inertial asteroseismology saw its birth thanks to high-precision
CoRoT and Kepler space photometric light curves. So far, it gave rise to the
internal rotation frequency of a few hundred intermediate-mass stars, yet only
several tens of these have been weighed, sized, and age-dated with high
precision from asteroseismic modelling. We aim to increase the sample of
optimal targets for future gravito-inertial asteroseismology by assessing the
properties of 15062 newly found Gaia DR3 gravity-mode pulsators. We also wish
to investigate if there is any connection between their fundamental parameters
and dominant mode on the one hand, and their spectral line broadening measured
by Gaia on the other hand. After re-classifying about 22% of the F-type
gravity-mode pulsators as B-type according to their effective temperature, we
construct histograms of the fundamental parameters and mode properties of the
15062 new Gaia DR3 pulsators. We compare these histograms with those of 63
Kepler bona fide class members. We fit errors-in-variables regression models to
couple the effective temperature, luminosity, gravity, and oscillation
properties to the two Gaia DR3 parameters capturing spectral line broadening
for a fraction of the pulsators. We find that the selected 15062 gravity-mode
pulsators have properties fully in line with those of their well-known Kepler
analogues, revealing that Gaia has a role to play in asteroseismology. The
dominant g-mode frequency is a significant predictor of the spectral line
broadening for the class members having this quantity measured. We show that
the Gaia vbroad parameter captures the joint effect of time-independent
intrinsic and rotational line broadening and time-dependent tangential
pulsational broadening. Gaia was not desiged to detect non-radial oscillations,
yet its homogeneous data treatment allow us to identify many new gravity-mode
pulsators.
