  We analyse a sample of 8 highly magnified galaxies at redshift 0.6<z<1.5
observed with MUSE, exploring the resolved properties of these galaxies at
sub-kiloparsec scales. Combining multi-band HST photometry and MUSE spectra, we
derive the stellar mass, global star formation rates, extinction and
metallicity from multiple nebular lines, concluding that our sample is
representative of z~1 star-forming galaxies. We derive the 2D kinematics of
these galaxies from the [OII] emission and model it with a new method that
accounts for lensing effects and fits multiple images simultaneously. We use
these models to calculate the 2D beam-smearing correction and derive intrinsic
velocity dispersion maps. We find them to be fairly homogeneous, with
relatively constant velocity dispersions between 15 - 80 km/s and Gini
coefficient of <0.3. We do not find any evidence for higher (or lower) velocity
dispersions at the positions of bright star-forming clumps. We derive resolved
maps of dust attenuation and attenuation-corrected star formation rates from
emission lines for two objects in the sample. We use this information to study
the relation between resolved star formation rate and velocity dispersion. We
find that these quantities are not correlated, and the high-velocity
dispersions found for relatively low star-forming densities seems to indicate
that, at sub-kiloparsec scales, turbulence in high-z discs is mainly dominated
by gravitational instability rather than stellar feedback.
