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The SgrB2 molecular cloud contains several sites forming high-mass stars.SgrB2(N) is one of its main centers of activity. It hosts several compact andUCHII regions, as well as two known hot molecular cores (SgrB2(N1) andSgrB2(N2)), where complex organic molecules are detected. Our goal is to usethe high sensitivity of ALMA to characterize the hot core population inSgrB2(N) and shed a new light on the star formation process. We use a complete3 mm spectral line survey conducted with ALMA to search for faint hot cores inSgrB2(N). We report the discovery of three new hot cores that we callSgrB2(N3), SgrB2(N4), and SgrB2(N5). The three sources are associated withclass II methanol masers, well known tracers of high-mass star formation, andSgrB2(N5) also with a UCHII region. The chemical composition of the sources andthe column densities are derived by modelling the whole spectra under theassumption of LTE. The H2 column densities are computed from ALMA and SMAcontinuum emission maps. The H2 column densities of these new hot cores arefound to be 16 up to 36 times lower than the one of the main hot core SgrB2(N1). Their spectra have spectral line densities of 11 up to 31 emissionlines per GHz, assigned to 22-25 molecules. We derive rotational temperaturesaround 140-180 K for the three new hot cores and mean source sizes of 0.4 forSgrB2(N3) and 1.0 for SgrB2(N4) and SgrB2(N5). SgrB2(N3) and SgrB2(N5) showhigh velocity wing emission in typical outflow tracers, with a bipolarmorphology in their integrated intensity maps suggesting the presence of anoutflow, like in SgrB2(N1). The associations of the hot cores with class IImethanol masers, outflows, and/or UCHII regions tentatively suggest thefollowing age sequence: SgrB2(N4), SgrB2(N3), SgrB2(N5), SgrB2(N1). The statusof SgrB2(N2) is unclear. It may contain two distinct sources, a UCHII regionand a very young hot core.

Exploring molecular complexity with ALMA (EMoCA): Detection of three new hot cores in Sagittarius B2(N)