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(Abridged) The recent measurement of the mass of two $2\, M_\odot$ pulsarshas raised the question whether such large masses allow for the existence ofexotic degrees of freedom, such as hyperons, inside neutron stars. In thepresent work we will investigate how the existing hypernuclei properties mayconstrain the neutron star equation of state and confront the neutron starmaximum masses obtained with equations of state calibrated to hypernucleiproperties with the astrophysical $2\,M_\odot$ constraint.  The study is performed using a relativistic mean field approach to describeboth the hypernuclei and the neutron star equations of state. A set of fivemodels consistent with $2\,M_\odot$ for a purely nucleonic composition areemployed. The $\Lambda$-meson couplings are determined for all the modelsconsidered. Hyperonic stars with the complete baryonic octet are studied,restricting the coupling of the $\Sigma$ and $\Xi$ hyperons to the $\omega-$,$\rho-$ and $\sigma-$mesons due to the lack of experimental data, and maximumstar masses calculated for unified equations of state. We conclude that thecurrently available hypernuclei experimental data and the lack of constraintson the asymmetric equation of state of nuclear matter at high densities do notallow to further constrain the neutron star matter equation of state using therecent $2\, M_\odot$ observations. It is also shown that the $\Lambda$potential in symmetric nuclear matter takes a value $\sim 30-32$ MeV atsaturation for the $g_{\omega \Lambda}$ coupling given by the SU(6) symmetry,close to values generally used in the literature. However, the $\Lambda$potential in $\Lambda$ matter varies between -16 and -8 MeV taking for vectormesons couplings the SU(6) values, at variance with generally employed valuesbetween $-1$ and $-5$ MeV.

(No) neutron star maximum mass constraint from hypernuclei