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In the seconds following their formation in core-collapse supernovae,"proto"-magnetars drive neutrino-heated magneto-centrifugal winds. Using asuite of two-dimensional axisymmetric MHD simulations, we show that relativelyslowly rotating magnetars with initial spin periods of $P_{\star0}=50-500$ msspin down rapidly during the neutrino Kelvin-Helmholtz cooling epoch. Theseinitial spin periods are representative of those inferred for normal Galacticpulsars, and much slower than those invoked for gamma-ray bursts andsuper-luminous supernovae. Since the flow is non-relativistic at early times,and because the Alfv\'en radius is much larger than the proto-magnetar radius,spindown is millions of times more efficient than the typically-used dipoleformula. Quasi-periodic plasmoid ejections from the closed zone enhancespindown. For polar magnetic field strengths $B_0\gtrsim5\times10^{14}$ G, thespindown timescale can be shorter than than the Kelvin-Helmholtz timescale. For$B_0\gtrsim10^{15}$ G, it is of order seconds in early phases. We compute thespin evolution for cooling proto-magnetars as a function of $B_0$,$P_{\star0}$, and mass ($M$). Proto-magnetars born with $B_0$ greater than$\simeq1.3\times10^{15}\,{\rm\,G}\,(P_{\star0}/{400\,\rm\,ms})^{-1.4}(M/1.4\,{\rmM}_\odot)^{2.2}$ spin down to periods $> 1$ s in just the first few seconds ofevolution, well before the end of the cooling epoch and the onset of classicdipole spindown. Spindown is more efficient for lower $M$ and for larger$P_{\star0}$. We discuss the implications for observed magnetars, including thediscrepancy between their characteristic ages and supernova remnant ages.Finally, we speculate on the origin of 1E 161348-5055 in the remnant RCW 103,and the potential for other ultra-slowly rotating magnetars.

The Early Evolution of Magnetar Rotation I: Slowly Rotating "Normal" Magnetars