Context :

Aims : We present an extended grid of state-of-the art stellar models for low-mass stars including updated physics ( nuclear reaction rates , surface boundary condition , mass-loss rate , angular momentum transport , torque and rotation-induced mixing prescriptions ) .
We aim at evaluating the impact of wind braking , realistic atmospheric treatment , rotation and rotation-induced mixing on the structural and rotational evolution from the pre-main sequence to the turn-off .

Methods : Using the STAREVOL code , we provide an updated PMS grid .
We compute stellar models for 7 different metallicities , from [ Fe/H ] = -1 dex to [ Fe/H ] = +0.3 dex with a solar composition corresponding to Z = 0.0134 .
The initial stellar mass ranges from 0.2 to 1.5 M _ { \odot } with extra grid refinement around one solar mass .
We also provide rotating models for three different initial rotation rates ( slow , median and fast ) with prescriptions for the wind braking and disc-coupling timescale calibrated on observed properties of young open clusters .
The rotational mixing includes an up-to-date description of the turbulence anisotropy in stably stratified regions .

Results : The overall behaviour of our models at solar metallicity – and its constitutive physics – is validated through a detailed comparison with a variety of distributed evolutionary tracks .
The main differences arise from the choice of surface boundary conditions and initial solar composition .
The models including rotation with our prescription for angular momentum extraction and self-consistent formalism for angular momentum transport are able to reproduce the rotation period distribution observed in young open clusters over a broad mass-range .
These models are publicly available and may be used to analyse data coming from present and forthcoming asteroseismic and spectroscopic surveys such as Gaia , TESS and PLATO .

Conclusions :