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We present the spectrophotometric properties of a sample of 141 emission-linegalaxies at redshifts in the range $0.2<z<1.0$ with a peak around$z\in[0.2,0.4]$. The analysis is based on medium resolution($R\_{\mathrm{s}}=500-600$), optical spectra obtained at VLT and Keck. Thetargets are mostly {} "Canada-France Redshift Survey" emission-line galaxies,with the addition of field galaxies randomly selected behind lensing clusters.We complement this sample with galaxy spectra from the {} "Gemini Deep DeepSurvey" public data release. We have computed absolute magnitudes of thegalaxies and measured the line fluxes and equivalent widths of the mainemission/absorption lines. The last two have been measured after carefulsubtraction of the fitted stellar continuum using the \texttt{platefit}software originally developed for the SDSS and adapted to our data. We presenta careful comparison of this software with the results of manual measurements.The pipeline has also been tested on lower resolution spectra, typical of the{} "VIMOS/VLT Deep Survey" ($R\_{\mathrm{s}}=250$), by resampling our mediumresolution spectra. We show that we can successfully deblend the most importantstrong emission lines. These data are primarily used to perform a spectralclassification of the galaxies in order to distinguish star-forming galaxiesfrom AGNs. Among the initial sample of 141 emission-line galaxies, we find 7Seyfert 2 (narrow-line AGN), 115 star-forming galaxies and 16 {} "candidate"star-forming galaxies. Scientific analysis of these data, in terms of chemicalabundances, stellar populations, etc, will be presented in subsequent papers ofthis serie.Comment: 24 pages. Accepted for publication in A&A; reference added; bug  corrected: flux scaled by (1+z

Spectrophotometric properties of galaxies at intermediate redshifts (z ~ 0.2–1.0)