We construct a set of hyperonic equations of state (EoS) by assuming SU(3)
symmetry within the baryon octet and by using a covariant density functional
(CDF) theory approach. The low-density regions of our EoS are constrained by
terrestrial experiments, while the high-density regime is modeled by
systematically varying the nuclear matter skewness coefficient ${Q}_{\mathrm{s}\mathrm{a}\mathrm{t}}$
and the symmetry energy slope ${L}_{\mathrm{s}\mathrm{y}\mathrm{m}}$ . The sensitivity of the EoS
predictions is explored in terms of $z$ parameter of the SU(3) symmetric model
that modifies the meson-hyperon coupling constants away from their SU(6)
symmetric values. Our results show that model EoS based on our approach can
support static Tolman-Oppenheimer-Volkof (TOV) masses in the range
$2.3$ -$2.5{\textstyle \phantom{\rule{0.167em}{0ex}}}{M}_{\odot}$ in the large-${Q}_{\mathrm{s}\mathrm{a}\mathrm{t}}$ and small-$z$ regime,
however, such stars contain only a trace amount of hyperons compared to SU(6)
models. We also construct uniformly rotating Keplerian configurations for our
model EoS for which the masses of stellar sequences may reach up to
$3.0{\textstyle \phantom{\rule{0.167em}{0ex}}}{M}_{\odot}$ . These results are used to explore the systematic dependence
of the ratio of maximum masses of rotating and static stars, the lower bound on
the rotational frequency of the models that will allow secondary masses in the
gravitational waves events to be compact stars with ${M}_{2}\lesssim 3.0{\textstyle \phantom{\rule{0.167em}{0ex}}}{M}_{\odot}$ and the strangeness fraction on the model parameters. We
conclude that very massive stellar models can be, in principle, constructed
within the SU(3) symmetric model, however, they are nucleonic-like as their
strangeness fraction drops below 3\%.