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We determine rotation periods for 127 stars in the ~115 Myr old Blanco 1 opencluster using ~200 days of photometric monitoring with the Next GenerationTransit Survey (NGTS). These stars span F5-M3 spectral types (1.2 $\gtrsim M\gtrsim$ 0.3 M$_{\odot}$) and increase the number of known rotation periods inBlanco 1 by a factor of four. We determine rotation periods using threemethods: Gaussian process (GP) regression, generalised autocorrelation (G-ACF)and Lomb-Scargle (LS) periodograms, and find that GPs and G-ACF are moreapplicable to evolving spot modulation patterns. Between mid-F and mid-Kspectral types, single stars follow a well-defined rotation sequence from ~2 to10 days, whereas stars in photometric multiple systems typically rotate faster.This may suggest that the presence of a moderate-to-high mass ratio companioninhibits angular momentum loss mechanisms during the early pre-main sequence,and this signature has not been erased at ~100 Myr. The majority of mid-F tomid-K stars display evolving modulation patterns, whereas most M stars showstable modulation signals. This morphological change coincides with the shiftfrom a well-defined rotation sequence (mid-F to mid-K stars) to a broadrotation period distribution (late-K and M stars). Finally, we compare ourrotation results for Blanco 1 to the similarly-aged Pleiades: the single starpopulations in both clusters possess consistent rotation period distributions,which suggests that the angular momentum evolution of stars follows awell-defined pathway that is, at least for mid-F to mid-K stars, stronglyimprinted by ~100 Myr.

NGTS clusters survey. I. Rotation in the young benchmark open cluster Blanco 1