  We selected 35 low-mass SFGs (7.9<log(M$_*$/M$_{\odot}$)<10.3) from deep
spectroscopic surveys based on their CIII]1908 emission. We used follow-up NIR
observations to examine their rest-optical emission lines and identify ionized
outflow signatures through broad emission wings detected after Gaussian
modeling of [OIII]4959,5007 profiles. We characterized the galaxies' gas-phase
metallicity and carbon-to-oxygen (C/O) abundance using a Te-based method via
the OIII]1666/[OIII]5007 ratio and photoionization models. We find line ratios
and rest-frame EWs characteristic of high-ionization conditions powered by
massive stars. Our sample displays mean rest-frame EW([OIII]5007)~560\r{A}
while 15% of them show EW([OIII]4959,5007)>1000\r{A} and EW(CIII])>5\r{A},
closely resembling those now seen in EoR galaxies with JWST. We find low
gas-phase metallicities 12+log(O/H)~7.5-8.5 and C/O abundances from 23%-128%
solar, with no apparent increasing trend with metallicity. From our
[OIII]4959,5007 profile modeling, we find that 65% of our sample shows an
outflow component, which is shifted relative to the ionized gas systemic
velocity, with mean $v_{max}$~280 km/s which correlates with the
$\Sigma_{SFR}$. We find that the mass-loading factor $\mu$ of our sample is
typically lower than in more massive galaxies from literature but higher than
in typical local dwarf galaxies. In the stellar mass range covered, we find
that $\mu$ increases with $\Sigma_{SFR}$ thus suggesting that for a given
stellar mass, denser starbursts in low-mass galaxies produce stronger outflows.
Our results complement the picture drawn by similar studies at lower redshift,
suggesting that the removal of ionized gas in low-mass SFGs driven by stellar
feedback is regulated by their stellar mass and by the strength and
concentration of their star formation, i.e. $\Sigma_{\rm SFR}$.
