Supernova feedback injects energy and turbulence, influencing the star formation process, and is therefore essential to understanding the formation and evolution of galaxies. Supernova remnants exhibit distinctive emission line ratios and kinematic signatures, which are apparent in optical spectroscopy. Using optical integral field unit data from PHANGS-MUSE collaboration project, we are able to identify supernova remnants within 19 nearby galaxies. We use a combination of five different optical diagnostics to identify SNRs. We account for the influence of diffuse ionized gas, using the line ratio maps of [SII]/Halpha and [OI]/Halpha in comparison with the Halpha surface brightness to select out supernova remnants. In addition, the velocity dispersion map and line ratio diagnostic diagrams are also useful ancillaries to confirm their identification. We identify 2399 supernova remnants within 19 nearby galaxies. This paper catalogs optical SNRs from PHANGS-MUSE and characterizes them. ~ 33% of SNRs lie within HII regions. In the five criteria we use to identify SNRs, in comparison with the Halpha surface brightness works best that select out 1482 SNRs. We also define a clean sample of 1276 SNRs that have been detected in at least two diagnostics, giving us high confidence in our characterization of these as SNRs. Overall, our detection of ~ 130 SNRs per galaxy implies an SN rate of 1~2 per century in our sample.