JADES-GS-z14-0 is the most distant spectroscopically confirmed galaxy so far,at $z>14$. With a UV magnitude of -20.81, it is one of the most luminousgalaxies at cosmic dawn and its half-light radius of 260 pc means that starsdominate the observed UV emission. We report the ALMA detection of[OIII]88$\mu$m line emission with a significance of 6.67$\sigma$ and at afrequency of 223.524 GHz, corresponding to a redshift of $14.1796\pm0.0007$,which is consistent with the candidate CIII] line detected in the NIRSpecspectrum. At this spectroscopic redshift, the Lyman break identified withNIRSpec requires a damped Lyman-$\alpha$ absorber with a column density of$\log(N_{\rm HI}/\mathrm{cm}^{-2})=22.23$. The total [OIII]88$\mu$m luminosity(log($(L_{\rm [OIII]}/L_\odot) = 8.3\pm0.1$) is fully consistent with the local$L_{\rm [OIII]}-SFR$ relation. Based on the ${L_{\rm [OIII]}/SFR}$, we infer agas-phase metallicity $>0.1~{\rm Z_{\rm \odot}}$, which is somewhat unexpectedgiven the weakness of the UV emission lines. Using prospector SED modeling andcombining the ALMA data with JWST observations, we find $Z=0.17~{Z_{\rm\odot}}$ and an escape fraction of ionizing photons of 20%, which is necessaryto explain the UV spectrum. We measure an [O III]5007\r{A}/[O III]88$\mu$m lineflux ratio between 1 and 10, resulting in an upper limit to the electrondensity of roughly 300 cm$^{-3}$, which is lower than those measured in otherhigh-$z$ luminous galaxies. The [OIII]88$\mu$m emission line is spectrallyresolved, with a FWHM of 100 km/s, resulting in a dynamical mass of$\log$(M$_{\rm dyn}/M_\odot$) = 9.0$\pm0.2$. This value is comparable to thestellar mass derived from the SED fitting, which implies a very low gasfraction. Past radiation-driven outflows may have cleared the galaxy from thegas, reducing the gas fraction and thus increasing the escape fraction ofionizing photons.