This study explores rotational signatures in 250 ultra-cool dwarfs (UCDs) from Gaia DR3 using TESS light curves. Clear periodic variability was found in 71 targets; 61 exhibit rotation with single-source behavior and periods ranging from 0.133 to 5.81 days. Five show double-dip features, and 10 likely represent non-single systems. Twenty UCDs display complex or irregular variability, while the remaining 159 show low-amplitude or noisy signals. In a color–magnitude diagram, two rotational regimes emerge: slower rotators (Prot ≥ 1.0 day) associated with less massive, younger late-M stars, and faster rotators (Prot < 1.0 day) with more massive, older early-M stars. Whether this distribution reflects physical processes or observational bias remains an open question.