  The Gaia mission has delivered hundreds of thousands of variable star light
curves in multiple wavelengths. Recent work demonstrates that these light
curves can be used to identify (non-)radial pulsations in the OBAF-type stars,
despite the irregular cadence and low light curve precision of order a few
mmag. With the considerably more precise TESS photometry, we revisit these
candidate pulsators to conclusively ascertain the nature of their variability.
We seek to re-classify the Gaia light curves with the first two years of TESS
photometry for a sample of 58,970 p- and g- mode pulsators, encompassing gamma
Dor, delta Scuti, SPB, and beta Cep variables. We also supply four new
catalogues containing the confirmed pulsators, along with their dominant and
secondary pulsation frequencies, the number of independent mode frequencies,
and a ranking according to their usefulness for future asteroseismic ensemble
analysis. We find that the Gaia photometry is exceptionally accurate for
detecting the dominant and secondary frequencies, reaching approximately 80%
accuracy in frequency for p- and g-mode pulsators. The majority of Gaia
classifications are consistent with the classifications from the TESS data,
illustrating the power of the low-cadence Gaia photometry for pulsation
studies. We find that the sample of g-mode pulsators forms a continuous group
of variable stars along the main sequence across B, A, and F spectral types,
implying that the mode excitation mechanisms for all these pulsators need to be
updated with improved physics. Finally, we provide a rank-ordered table of
pulsators according to their asteroseismic potential for follow-up studies. Our
catalogue offers a major increase in the number of confirmed gravity-mode
pulsators with an identified dominant mode suitable for follow-up TESS ensemble
asteroseismology of such stars.
