We discuss the chemical properties of a sample of UV-selected intermediate-redshift (0 < z < 0.4) galaxies in the context of their physical nature and star formation history. This work represents an extension of our previous studies (Treyer et al. 1998; Sullivan et al. 2000, 2001) on UV-selected galaxies. We revisit the optical spectra of these galaxies and perform further emission-line measurements restricting the analysis to those spectra with the full set of emission lines required to derive chemical abundances. Our final sample consists of 68 galaxies with heavy element abundance ratios and both UV and CCD B-band photometry. Diagnostics based on emission-line ratios show that all but one of the galaxies in our sample are powered by hot, young stars rather than by an AGN. Oxygen-to-hydrogen (O/H) and nitrogen-to-oxygen (N/O) abundance ratios are compared to those for various local and intermediate-redshift samples. Our UV-selected galaxies span a wide range of oxygen abundances, from 0.1 Zsun to solar, intermediate between low-mass HII galaxies and massive starburst nuclei. For a given oxygen abundance, most have strikingly low N/O values. Moreover, UV-selected and HII galaxies systematically deviate from the usual metallicity-luminosity relation in the sense of being more luminous by 2-3 magnitudes. Adopting the "delayed-release" chemical evolution model, we propose our UV-selected sources are observed at a special stage in their evolution, following a powerful starburst which enriched their ISM in oxygen and temporarily lowered their mass-to-light ratios. We discuss briefly the implications of our conclusions on the nature of similarly-selected high-redshift galaxies.

17 pages, 10 figures, and 2 tables. Accepted for publication in MNRAS