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We present optical and near-IR imaging and spectroscopy of SGASJ105039.6$+$001730, a strongly lensed galaxy at z $=$ 3.6252 magnified by$>$30$\times$, and derive its physical properties. We measure a stellar mass oflog(M$_{*}$/M$_{\odot}$) $=$ 9.5 $\pm$ 0.35, star formation rates from [OII]$\lambda$$\lambda$3727 and H-$\beta$ of 55 $\pm$ 20 and 84 $\pm$ 17M$_{\odot}$ yr$^{-1}$, respectively, an electron density of n$_{e} \leq$10$^{3}$ cm$^{-2}$, an electron temperature of T$_{e} \leq$ 14000 K, and ametallicity of 12+log(O/H) $=$ 8.3 $\pm$ 0.1. The strong CIII]$\lambda$$\lambda$1907,1909 emission and abundance ratios of C, N, O and Siare consistent with well-studied starbursts at z $\sim$ 0 with similarmetallicities. Strong P Cygni lines and He II$\lambda$1640 emission indicate asignificant population of Wolf-Rayet stars, but synthetic spectra of individualpopulations of young, hot stars do not reproduce the observed integrated PCygni absorption features. The rest-frame UV spectral features are indicativeof a young starburst with high ionization, implying either 1) an ionizationparameter significantly higher than suggest by rest-frame optical nebularlines, or 2) differences in one or both of the initial mass function and theproperties of ionizing spectra of massive stars. We argue that the observedfeatures are likely the result of a superposition of star forming regions withdifferent physical properties. These results demonstrate the complexity of starformation on scales smaller than individual galaxies, and highlight theimportance of systematic effects that result from smearing together thesignatures of individual star forming regions within galaxies.

The Physical Conditions, Metallicity and Metal Abundance Ratios In a Highly Magnified Galaxy at z = 3.6252