  Recent astrophysical mass inferences of compact stars HESS J1731-347 and PSR
J0952-0607, with extremely small and large masses respectively, as well as the
measurement of the neutron skin of Ca in the CREX experiment challenge and
constrain the models of dense matter. We examine the concept of hybrid stars -
objects containing quark cores surrounded by nucleonic envelopes - as models
that account for these new data along with other inferences. We employ a family
of 81 nucleonic equations of state (EoSs) with variable skewness and slope of
symmetry energy at saturation density and a constant speed-of-sound EoS for
quark matter. For each nucleonic EoS, a family of hybrid EoSs is generated by
varying the transition density, the energy jump, and the speed of sound. These
models are tested against the data from GW170817 and J1731-347, which favor
low-density soft EoS and J0592-0607 and J0740+6620, which require high-density
stiff EoS. The addition of J0592-0607's mass measurement to the constraints has
no significant impact on the parameter space of the admissible EoS, but allows
us to explore the potential effect of pulsars more massive than J0740+6620, if
such exists. We then examine the occurrence of twin configurations and quantify
the ranges of masses and radii that they can possess. It is shown that
including J1731-347 data favors EoSs that predict low-mass twins with $M
\lesssim 1.3\,M_{\odot}$ that can be realized if the deconfinement transition
density is low. If combined with large speed of sound in quark matter such
models allow for maximum masses of hybrid stars in $2.0$--$2.6\,M_{\odot}$.
