  We present a study of high-cadence, high-precision, optical light curves from
the TESS satellite of 67 blazars in the southern sky. We provide descriptive
flux statistics, power spectral density model parameters, and characteristic
variability timescales. We find that only 15 BL Lacertae objects (BLLs) and 18
Flat Spectrum Radio Quasars (FSRQs) from the initial 26 and 41, respectively
exhibit statistically-significant variability. We employ an adapted Power
Spectral Response method to test the goodness of fit for the power spectral
density function (PSD) to 3 power-law variant models. From our best-fitting
description of the PSD, we extract the high-frequency power-spectral slopes
and, if present, determine the significant bend or break in the model to
identify characteristic timescales. We find no significant difference in the
excess variance or rms-scatter between blazar subpopulations. We identify a
linear rms-flux relation in ~69% of our sample, in which ~20% show a strong
correlation. We find that both subpopulations of blazars show power spectral
slope of $\alpha$~2 in which a broken power-law best fits 5 BLL & 6 FSRQ and a
bending power-law best fits 1 BLL & 5 FSRQ. The shortest timescales of
variability in each light curve range widely from minutes to weeks.
Additionally, the objects' characteristic timescales range from ~0.8-8 days,
consistent with the optical variability originating in the jet.
