We map the observational predictions of cosmological stasis in the inflationary gravitational wave background (IGWB) onto the sensitivity bands of current and planned gravitational wave detectors. Using the closed-form piecewise spectral template derived in the companion paper~, we generate detectability maps for four stasis scenarios — canonical ($0\le w_s<1/3$), stiff ($1/3<w_s<1$), vacuum-energy/matter ($-1/3<w_s<0$), and vacuum-energy/radiation ($-1/3<w_s<1/3$) — across the frequency bands probed by NANOGrav, SKA, LISA, DECIGO, BBO, the Einstein Telescope, and Cosmic Explorer. For scenarios in which the spectrum is suppressed, $w_s<1/3$, the stasis feature is detectable by BBO in the region of $(w_s,\Delta N)$ parameter space in which $w_s\gtrsim 0.2$ for tensor-to-scalar ratios close to the Planck upper limit, r = 0.036, while to be detectable by DECIGO requires $w_s\gtrsim 0.3$. For scenarios in which the spectrum is enhanced, $w_s>1/3$, the stasis feature is detectable by BBO across the entire $(w_s,\Delta N)$ parameter space for tensor-to-scalar ratios of $O(0.01)$. For large values of $w_s$ close to the kination limit, the feature is detectable for r as small as ${10}^{-9}$. We characterize the Standard-Model (SM) $g_{*}$ fine structure of the IGWB, showing that SM phase transitions introduce spectral steps of $\approx 20\%$ (electroweak, at $\sim 2.6\times {10}^{-6}$~Hz) and $\approx 53\%$ (QCD, at $\sim 3.6\times {10}^{-9}$~Hz). For stasis scenarios with end-of-stasis temperatures below the QCD scale these steps fall inside the stasis band and constitute additional spectral features that complement the primary signature. Finally, we model the finite-width end-of-stasis transition phenomenologically, demonstrating that the spectral break at $\fend$ is smoothed over a log-frequency window $\Delta N_{trans}\times 3(1+w_s)/4$, and that the consistency relation $\Ccal^2=\Ccal^2(\alpha)$ remains testable provided $\Delta N_{stasis}\gg \Delta N_{trans}$, a condition easily satisfied for all scenarios of phenomenological interest.