  Compact radio jets are ubiquitous in stellar-mass black-hole binaries in
their hard spectral state. Empirical relations between the radio and
narrow-band X-ray fluxes have been used to understand the connection between
their accretion discs and jets. However, a narrow-band (e.g., 1--10 or 3--9
keV) X-ray flux can be a poor proxy for either the bolometric luminosity or the
mass accretion rate. Here, we study correlations between the radio and
unabsorbed broad-band X-ray fluxes, the latter providing good estimates of the
bolometric flux. We consider GX 339--4, the benchmark object for the main
branch of the correlation, and H1743--322, the first source found to be an
outlier of the correlation. The obtained power-law dependencies of the radio
flux on the bolometric flux have significantly different indices from those
found for the narrow X-ray bands. Also, the radio/bolometric flux correlations
for the rise of the outbursts are found to be significantly different from
those for the outburst decline. This points to a possible existence of a jet
hysteresis in the radio/X-ray source evolution, in addition to that seen in the
hardness/flux diagram of low-mass X-ray binaries. The correlation during the
rise of the outbursts is similar for both GX 339--4 and H1743--322. The
correlation for the decline of the outbursts for H1743--322 lies below that of
GX 339--4 at intermediate X-ray fluxes, whereas it approaches the standard
correlation at lower X-ray luminosities. We also compare these correlations to
those for the high-mass X-ray binaries Cyg X-1 and Cyg X-3.
