Comparison of the period distributions obtained for various young clusters of different ages, in the mass range 0.1–2 M_⊙. The clusters are, from left to right, from top to bottom: NGC 6530 (age of ~2 Myr, Bell et al. 2013; periods from Henderson & Stassun 2012; 241 objects with measured rotation periods in the mass range of interest here); the Orion Nebula Cluster (ONC; age in the range 2.8–5.2 Myr, Naylor 2009; rotation periods from Rodríguez-Ledesma et al. 2009 for objects with M_⋆ < 0.4 M_⊙, and from Irwin & Bouvier 2009, after Herbst et al. 2001, 2002 and Stassun et al. 1999, for objects with M_⋆ > 0.4 M_⊙; 528 objects with measured periods in the selected mass range); NGC 2264 (age in the range 2.4–6 Myr, Naylor 2009; period measurements reported in this study; 272 objects); Cepheus OB3b (age of ~6 Myr, Bell et al. 2013; periods from Littlefair et al. 2010; 460 objects with period measurements in the selected mass range); NGC 2362 (age in the range 9.5–12.6 Myr, Bell et al. 2013; periods from Irwin et al. 2008; 272 objects with periods in the mass range of interest); h Persei (age of ~13 Myr, Mayne & Naylor 2008; periods from Moraux et al. 2013; 586 objects with measured periods in the selected mass range).