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Sigma Ori E, a massive helium B-type star, shows a high surface rotation anda strong surface magnetic field potentially challenging the process of windmagnetic braking. The Gaia satellite provides an accurate distance to that starand confirms its membership to the sigma Ori cluster. We account for these twokey pieces of information to investigate whether single star models canreproduce the observed properties of sigma Ori E and provide new estimates forits metallicity, mass, and age. We compute rotating stellar models accountingfor wind magnetic braking and magnetic quenching of the mass loss. We obtainthat sigma Ori E is a very young star (age less than 1 Myr) with an initialmass around 9 Msol, a surface equatorial magnetic field around 7 kG and havinga metallicity Z (mass fraction of heavy elements) around 0.020. No solution isobtained with the present models for a metallicity Z=0.014. The initialrotation of the models fitting sigma Ori E is not much constrained and can beanywhere in the range studied in the present work. Because of its very youngage, models predict no observable changes of the surface abundances due torotational mixing. The simultaneous high surface rotation and high surfacemagnetic field of sigma Ori E may simply be a consequence of its young age.This young age implies that the processes responsible for producing thechemical inhomogeneities that are observed at its surface should be rapid. Thusfor explaining the properties of sigma Ori E, there is no necessity to invoke amerging event although such a scenario cannot be discarded. Other stars (HR5907, HR 7355, HR 345439, HD 2347, CPD -50^{o}3509$) showing similar propertiesas sigma Ori E (fast rotation and strong surface magnetic field) may also bevery young stars, although determination of the braking timescales is needed toconfirm such a conclusion.

News from Gaia on sigma Ori E: a case study for the wind magnetic braking process