  Spinning supermassive black holes (BHs) in active galactic nuclei (AGN)
magnetically launch relativistic collimated outflows, or jets. Without angular
momentum supply, such jets are thought to perish within $3$ orders of magnitude
in distance from the BH, well before reaching kpc-scales. We study the survival
of such jets at the largest scale separation to date, via 3D general
relativistic magnetohydrodynamic simulations of rapidly spinning BHs immersed
into uniform zero-angular-momentum gas threaded by weak vertical magnetic
field. We place the gas outside the BH sphere of influence, or the Bondi
radius, chosen much larger than the BH gravitational radius,
$R_\text{B}=10^3R_\text{g}$. The BH develops dynamically-important large-scale
magnetic fields, forms a magnetically-arrested disk (MAD), and launches
relativistic jets that propagate well outside $R_\text{B}$ and suppress BH
accretion to $1.5\%$ of the Bondi rate, $\dot{M}_\text{B}$. Thus,
low-angular-momentum accretion in the MAD state can form large-scale jets in
Fanaroff-Riley (FR) type I and II galaxies. Subsequently, the disk shrinks and
exits the MAD state: barely a disk (BAD), it rapidly precesses, whips the jets
around, globally destroys them, and lets $5-10\%$ of $\dot{M}_\text{B}$ reach
the BH. Thereafter, the disk starts rocking back and forth by angles
$90-180^\circ$: the rocking accretion disk (RAD) launches weak intermittent
jets that spread their energy over a large area and suppress BH accretion to
$\lesssim 2 \% ~ \dot{M}_\text{B}$. Because BAD and RAD states tangle up the
jets and destroy them well inside $R_\text{B}$, they are promising candidates
for the more abundant, but less luminous, class of FR0 galaxies.
