  We present Atacama Large Millimeter/submillimeter Array (ALMA) resolved
observations of molecular gas in galaxies up to $z=0.35$ to characterise the
role of global galactic dynamics on the global interstellar medium (ISM)
properties. These observations consist of a sub-sample of 39 galaxies taken
from the Valpara\'iso ALMA Line Emission Survey (VALES). From the CO($J=1-0)$
emission line, we quantify the kinematic parameters by modelling the velocity
fields. We find that the IR luminosity increases with the rotational to
dispersion velocity ratio ($V_{\rm rot}/\sigma_v$, corrected for inclination).
We find a dependence between $V_{\rm rot}/\sigma_v$ and the [CII]/IR ratio,
suggesting that the so-called `[CII] deficit' is related to the dynamical state
of the galaxies. We find that global pressure support is needed to reconcile
the dynamical mass estimates with the stellar masses in our systems with low
$V_{\rm rot}/\sigma_v$ values. The star formation rate (SFR) is weakly
correlated with the molecular gas fraction ($f_{\rm H_2}$) in our sample,
suggesting that the release of gravitational energy from cold gas may not be
the main energy source of the turbulent motions seen in the VALES galaxies. By
defining a proxy of the `star formation efficiency' parameter as the SFR
divided by the CO luminosity (SFE$'\equiv$ SFR/L$'_{\rm CO}$), we find a
constant SFE$'$ per crossing time ($t_{\rm cross}$). We suggest that $t_{\rm
cross}$ may be the controlling timescale in which the star formation occurs in
dusty $z\sim0.03-0.35$ galaxies.
