  We study 119 B stars located in the Scorpius-Centaurus Association using data
from NASA's TESS Mission. We see pulsations in 81 stars (68%) across the full
range of effective temperatures. In particular, we confirm previous reports of
low-frequency pulsations in stars whose temperatures fall between the
instability strips of SPB stars (slowly pulsating B stars) and $\delta$ Scuti
stars. By taking the stellar densities into account, we conclude that these
cannot be p modes and confirm previous suggestions that these are probably
rapidly-rotating SPB stars. We also confirm that they follow two
period-luminosity relations that are consistent with prograde sectoral g modes
that are dipole ($l=m=1$) and quadrupole ($l=m=2$), respectively. One of the
stars ($\xi^2$ Cen) is a hybrid pulsator that shows regular spacings in both g
and p modes. We confirm that $\alpha$ Cru has low-amplitude p-mode pulsations,
making it one of the brightest $\beta$ Cephei stars in the sky. We also find
several interesting binaries, including a very short-period heartbeat star (HD
132094), a previously unknown eclipsing binary ($\pi$ Lup), and an eclipsing
binary with high-amplitude tidally driven pulsations (HR 5846). The results
clearly demonstrate the power of TESS for studying variability in stellar
associations.
