  Lynds 1340, a molecular cloud forming intermediate-mass stars, has been
mapped in the NH_3(1,1) and (2,2) transitions with the Effelsberg 100m
telescope. We observed the whole area of the cloud where C18O emission was
detected earlier, at a 40 arcsec grid, with additional positions towards the
C18O peaks and optically invisible IRAS point sources. Our observations covered
an area of 170 arcmin^2, corresponding to about 5.15 pc^2 at a distance of 600
pc, and revealed 10 ammonia cores. The cores, occupying some 7% of the mapped
area, probably represent the highest density regions of L1340. Their total mass
is 80 solar mass, about 6% of the mass traced by C18O. Six cores are associated
with optically invisible IRAS point sources. Their average nonthermal line
width is 0.78 kms^{-1}, while the same quantity for the four starless cores is
0.28 kms^{-1}. We suggest that the narrow-line cores are destined to form
low-mass stars, whereas small groups of intermediate-mass stars are being
formed in the turbulent cores. The features traced by NH_3, 13CO, C18O and HI
obey the line width-size relation log Delta v_{NT} = 0.41(0.06)log R_{1/2}+
0.12(0.06). Comparison of sizes, densities and nonthermal line widths of
ammonia cores with those of C18O and 13CO structures supports the scenario in
which core formation has been induced by turbulent fragmentation. The typical
physical properties of the ammonia cores of L1340, R_{1/2} =0.08 pc,
T_{kin}=13.8 K, Delta v_{total}=0.64 kms^{-1}, and M =9 solar mass are close to
those of the high-mass star forming Perseus and Orion B clouds.
