  We report periods for 33 members of Blanco 1 as measured from KELT-South
light curves, the first reported rotation periods for this benchmark
zero-age-main-sequence open cluster. The distribution of these stars spans from
late-A or early-F dwarfs to mid-K with periods ranging from less than a day to
~8 days. The rotation period distribution has a morphology similar to the
coeval Pleiades cluster, suggesting the universal nature of stellar rotation
distributions. Employing two different gyrochronology methods, we find an age
of 146+13-14 Myr for the cluster. Using the same techniques, we infer an age of
134+9-10 Myr for the Pleiades measured from existing literature rotation
periods. These rotation-derived ages agree with independently determined
cluster ages based on the lithium depletion boundary technique. Additionally,
we evaluate different gyrochronology models, and quantify levels of agreement
between the models and the Blanco 1/Pleiades rotation period distributions,
including incorporating the rotation distributions of clusters at ages up to
1.1 Gyr. We find the Skumanich-like spin-down rate sufficiently describes the
rotation evolution of stars hotter than the Sun; however, we find cooler stars
rotating faster than predicted by a Skumanich-law, suggesting a mass dependence
in the efficiency of stellar angular momentum loss rate. Finally, we compare
the Blanco 1 and Pleiades rotation period distributions to available non-linear
angular momentum evolution models. We find they require a significant mass
dependence on the initial rotation rate of solar-type stars to reproduce the
observed range of rotation periods at a given stellar mass, and are furthermore
unable to predict the observed over-density of stars along the upper-envelope
of the clusters' rotation distributions.
