  Extreme-ultraviolet and X-ray jets occur frequently in magnetically open
coronal holes on the Sun, especially at high solar latitudes. Some of these
jets are observed by white-light coronagraphs as they propagate through the
outer corona toward the inner heliosphere, and it has been proposed that they
give rise to microstreams and torsional Alfv\'{e}n waves detected in situ in
the solar wind. To predict and understand the signatures of coronal-hole jets,
we have performed a detailed statistical analysis of such a jet simulated with
an adaptively refined magnetohydrodynamics model. The results confirm the
generation and persistence of three-dimensional, reconnectiondriven magnetic
turbulence in the simulation. We calculate the spatial correlations of magnetic
fluctuations within the jet and find that they agree best with the M\"{u}ller -
Biskamp scaling model including intermittent current sheets of various sizes
coupled via hydrodynamic turbulent cascade. The anisotropy of the magnetic
fluctuations and the spatial orientation of the current sheets are consistent
with an ensemble of nonlinear Alfv\'{e}n waves. These properties also reflect
the overall collimated jet structure imposed by the geometry of the
reconnecting magnetic field. A comparison with Ulysses observations shows that
turbulence in the jet wake is in quantitative agreement with that in the fast
solar wind.
