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The chemical inventory of planets is determined by the physical and chemicalprocesses that govern the early phases of star formation. The aim is toinvestigate N-bearing complex organic molecules towards two Class 0 protostars(B1-c and S68N) at millimetre wavelengths with ALMA. Next, the results of thedetected N-bearing species are compared with those of O-bearing species for thesame and other sources. ALMA observations in Band 6 ($\sim$ 1 mm) and Band 5($\sim$ 2 mm) are studied at $\sim$ 0.5" resolution, complemented by Band 3($\sim$ 3 mm) data in a $\sim$ 2.5" beam. NH2CHO, C2H5CN, HNCO, HN13CO, DNCO,CH3CN, CH2DCN, and CHD2CN are identified towards the investigated sources.Their abundances relative to CH3OH and HNCO are similar for the two sources,with column densities that are typically an order of magnitude lower than thoseof O-bearing species. The largest variations, of an order of magnitude, areseen for NH2CHO abundance ratios with respect to HNCO and CH3OH and do notcorrelate with the protostellar luminosity. In addition, within uncertainties,the N-bearing species have similar excitation temperatures to those ofO-bearing species ($\sim$ 100 $\sim$ 300 K). The similarity of most abundanceswith respect to HNCO, including those of CH2DCN and CHD2CN, hints at a sharedchemical history, especially the high D/H ratio in cold regions prior to starformation. However, some of the variations in abundances may reflect thesensitivity of the chemistry to local conditions such as temperature (e.g.NH2CHO), while others may arise from differences in the emitting areas of themolecules linked to their different binding energies in the ice. The twosources discussed here add to the small number of sources with such a detailedchemical analysis on Solar System scales. Future JWST data will allow a directcomparison between the ice and gas abundances of N-bearing species.

Complex organic molecules in low-mass protostars on Solar System scales -- II. Nitrogen-bearing species