  We report a new microscopic equation of state (EOS) of dense symmetric
nuclear matter, pure neutron matter, and asymmetric and $\beta$-stable nuclear
matter at zero temperature using recent realistic two-body and three-body
nuclear interactions derived in the framework of chiral perturbation theory
(ChPT) and including the $\Delta(1232)$ isobar intermediate state. This EOS is
provided in tabular form and in parametrized form ready for use in numerical
general relativity simulations of binary neutron star merging. Here we use our
new EOS for $\beta$-stable nuclear matter to compute various structural
properties of non-rotating neutron stars.The EOS is derived using the
Brueckner--Bethe--Goldstone quantum many-body theory in the
Brueckner--Hartree--Fock approximation. Neutron star properties are next
computed solving numerically the Tolman--Oppenheimer--Volkov structure
equations. Our EOS models are able to reproduce the empirical saturation point
of symmetric nuclear matter, the symmetry energy $E_{sym}$, and its slope
parameter $L$ at the empirical saturation density $n_{0}$. In addition, our EOS
models are compatible with experimental data from collisions between heavy
nuclei at energies ranging from a few tens of MeV up to several hundreds of MeV
per nucleon. These experiments provide a selective test for constraining the
nuclear EOS up to $\sim 4 n_0$. Our EOS models are consistent with present
measured neutron star masses and particularly with the mass $M = 2.01 \pm 0.04
\, M_{\odot}$ of the neutron stars in PSR~J0348+0432.
