  {\delta} Scuti variables are found at the intersection of the classical
instability strip and the main sequence on the Hertzsprung-Russell diagram.
With space-based photometry providing millions of light-curves of A-F type
stars, we can now probe the occurrence rate of {\delta} Scuti pulsations in
detail. Using 30-min cadence light-curves from NASA's Transiting Exoplanet
Survey Satellite's (TESS) first 26 sectors, we identify variability in 103,810
stars within 5-24 cycles per day down to a magnitude of $T=11.25$. We fit the
period-luminosity relation of the fundamental radial mode for {\delta} Scuti
stars in the Gaia $G$-band, allowing us to distinguish classical pulsators from
contaminants for a subset of 39,367 stars. Out of this subset, over 15,918 are
found on or above the expected period-luminosity relation. We derive an
empirical red edge to the classical instability strip using Gaia photometry.
The center where pulsator fraction peaks at 50-70%, combined with the red edge,
agree well with previous work in the Kepler field. While many variable sources
are found below the period-luminosity relation, over 85% of sources inside of
the classical instability strip derived in this work are consistent with being
{\delta} Scuti stars. The remaining 15% of variables within the instability
strip are likely hybrid or {\gamma} Doradus pulsators. Finally, we discover
strong evidence for a correlation between pulsator fraction and spectral line
broadening from the Radial Velocity Spectrometer (RVS) aboard the Gaia
spacecraft, confirming that rotation has a role in driving pulsations in
{\delta} Scuti stars.
