  TESS photometry is analyzed for 432 classical Be stars observed in the first
year of the mission. The often complex and diverse variability of each object
in this sample is classified to obtain an understanding of the behavior of this
class as a population. 98\% of the systems are variable above the noise level,
with timescales spanning nearly the entire range of what is accessible with
TESS, from tens of minutes to tens of days. The variability seen with TESS is
summarized as follows. Nearly every system contains multiple periodic signals
in the frequency regime between about 0.5 -- 4 d$^{-1}$. One or more groups of
closely-spaced frequencies is the most common feature, present in 85\% of the
sample. Among the Be stars with brightening events that are characteristic of
mass ejection episodes (17\% of the full sample, or 30\% of early-type stars),
all have at least one frequency group, and the majority of these (83\%) show a
concurrent temporary amplitude enhancement in one or more frequency groups.
About one third of the sample is dominated by low frequency ($f < 0.5$
d$^{-1}$, and often much lower) variability. Stochastic signals are prominent
in about 26\% of the sample, with varying degrees of intensity. Higher
frequency signals ($6 < f < 15$ d$^{-1}$) are sometimes seen (in 14\% of the
sample) and in most cases likely reflect p mode pulsation. In rare cases
($\sim$3\%), even higher frequencies beyond the traditional p mode regime ($f >
15$ d$^{-1}$) are observed.
