  We use the Spitzer Survey of Stellar Structure in Galaxies (S$^{4}$G) 3.6
$\mu$m imaging to study the properties (length and strength) and fraction of
bars at $z=0$. We use the maximum of tangential-to-radial force ratio in the
bar region ($Q_{\rm b}$) as a measure of the bar induced perturbation strength
for a sample of $\sim 600$ barred galaxies. Bars are also characterized from
the maximum of the normalized m=2 Fourier density amplitude ($A_{2}^{\rm max}$)
and the bar maximum isophotal ellipticity ($\varepsilon$). Combining our force
calculations with the HI kinematics from the literature we get an estimate of
the halo-to-stellar mass ratios ($M_{\rm h}/M_{\ast}$) within the optical disk,
which are in good agreement with studies based on weak lensing analysis,
abundance matching and halo occupation distribution methods. By further using
the Universal Rotation Curve models we obtain a first-order model of the
rotation curve decomposition of $1128$ disk galaxies. We find that the dilution
of $Q_{\rm b}$ by the halo becomes important for later types, implying $\sim
20-25\%$ reduction for $T = 7-10$. Whether the halo correction is included or
not, the mean $Q_{\rm b}$ shows an increasing trend with $T$. Late-type bars
are longer than previously found in the literature. We find possible evidence
for the growth of bars within a Hubble time, as (1) bars in early-type galaxies
show larger density amplitudes and disk-relative sizes than their
intermediate-type counterparts, and (2) long bars are typically strong. We also
observe two clearly distinct types of bars, between early and intermediate-type
galaxies ($T<5$) on one side, and the late-type systems on the other, based on
the differences in the bar properties. Most likely this distinction is
connected to the larger halo-to-stellar ratio that we observe in later types,
affecting the disk stability properties (Abridged).
