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We analyze the gas mass distribution, the gas kinematics, and the youngstellar object (YSO) content of the California Molecular Cloud (CMC) L1482filament. We derive a Gaia DR2 YSO distance of 511$^{+17}_{-16}$ pc. We derivescale-free power-laws for the mean gas line-mass (M/L) profiles; we calculatethe gravitational potential and field profiles consistent with these. Wepresent IRAM 30 m C$^{18}$O (1-0) (and other tracers) position-velocity (PV)diagrams that exhibit complex velocity twisting and turning structures. We finda rotational profile in C$^{18}$O perpendicular to the southern filamentridgeline. The profile is regular, confined ($r\lesssim0.4$ pc),anti-symmetric, and to first order linear with a break at $r\sim0.25$ pc. Thetimescales of the inner (outer) gradients are $\sim$0.7 (6.0) Myr. We show thatthe centripetal force, compared to gravity, increases toward the break; whenthe ratio of forces approaches unity, the profile turns over, just beforefilament breakup is achieved. The timescales and relative roles of gravity torotation indicate that the structure is stable, long lived ($\sim$ a few times6 Myr), and undergoing outside-in evolution. Moreover, this filament haspractically no star formation, a perpendicular Planck plane-of-the-sky (POS)magnetic field morphology, and POS "zig-zag" morphology, which together withthe rotation profile lead to the suggestion that the 3D shape is a corkscrewfilament with a helical magnetic field. These results, combined with results inOrion and G035.39-00.33, suggest evolution toward higher densities as rotatingfilaments shed angular momentum. Thus, magnetic fields may be an essentialfeature of high-mass (M $\sim10^5$ M$_{\odot}$) cloud filament evolution towardcluster formation.

Filament rotation in the California L1482 cloud