We quantify the stellar rotation of galaxies by computing the {lambda}_R_ parameter, a proxy for the stellar angular momentum in a sample of 106 intermediate-redshift galaxies (0.1<z<0.8). The sample is located in the CANDELS/GOODS-S and CANDELS/COSMOS regions, and it was observed by various MUSE surveys. We created spatially resolved stellar velocity and velocity dispersion maps using a full-spectrum fitting technique, covering spatially ~2Re for the galaxies. The sample spans stellar masses from ~10^7.5^M_{sun}_ to 10^11.8^M_{sun}_ with star formation rates (SFRs) from log10(SFR)~-3M_{sun}_/yr to ~1.7M_{sun}_/yr over a range of 6Gyr in cosmic time. We studied how the atmospheric seeing, introduced by the instrumental point spread function (PSF), affects the measured spin parameter, and we applied corrections when pertinent. Through the analysis of the {lambda}_R_-{epsilon} diagram, we note that the fraction of round and massive galaxies increases with redshift. We did not measure any galaxy with {lambda}_R_<0.1 in the sample, and we found only one potential (but uncertain) low-mass slow rotator at z~0.3, more similar to the z=0 low-mass slow rotators characterized by counter-rotation than to massive ellipticals. Moreover, we do not see an evident evolution or trend in the stellar angular momentum with redshift. We characterized the galaxy environment using two different indicators: a local estimator based on the Voronoi tesselation method, and a global estimator derived by the use of the friends-of-friends (FoF) algorithm. We find no correlation between the environment and {lambda}_R_ given that we are not probing dense regions or massive galaxy structures. We also analysed the kinematic maps of the sample finding that about 40% of the galaxies are consistent with being regular rotators (RRs), having rotating stellar discs with flat velocity dispersion maps, while ~20% have complex velocity maps and can be identified as non-regular rotators in spite of their {lambda}_R_ values. For the remaining galaxies the classification is uncertain. As we lack galaxies with {lambda}_R_<0.1 in the sample, we are not able to identify when galaxies lose their angular momentum and become slow rotators within the surveyed environments, area, and redshift range.