  Thin stellar streams originating from globular clusters are among the most
sensitive tracers of low-mass dark-matter subhalos. Joint analysis of the
entire population of stellar streams will place the most robust constraints on
the dark-matter subhalo mass function, and therefore the nature of dark matter.
Here we use a hierarchical model of globular cluster formation to forecast the
total number, masses and radial distribution of dissolved globular cluster in
Milky Way-like galaxies. Furthermore, we generate mock stellar streams from
these progenitors' orbital histories taking into account the clusters'
formation and accretion time, mass, and metallicity. Out of $\sim$10,000
clusters more massive than $10^4$ M$_{\odot}$, $\sim$9000 dissolved in the
central bulge and are fully phase-mixed at the present, while the remaining
$\sim$1000 survive as coherent stellar streams. This suggests that the current
census of $\sim$80 globular cluster streams in the Milky Way is severely
incomplete. Beyond 15 kpc from the Galactic center we are missing hundreds of
streams, of which the vast majority are from accreted GCs. Deep Rubin
photometry $(g\lesssim27.5)$ would be able to detect these streams, even the
most distant ones beyond $> 75$ kpc. We also find that M31 will have an
abundance of streams at galactocentric radii of 30-100 kpc. We conclude that
future surveys will find a multitude of stellar streams from globular clusters
which can be used for dark matter subhalo searches.
